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Stellar-mass Black Holes in Globular Clusters: Dynamical consequences and observational signatures

Published online by Cambridge University Press:  11 March 2020

Abbas Askar Open the ORCID record for Abbas Askar [Opens in a new window] ,
Mirek Giersz Open the ORCID record for Mirek Giersz [Opens in a new window] ,
Manuel Arca Sedda ,
Ammar Askar ,
Mario Pasquato  and
Agostino Leveque Open the ORCID record for Agostino Leveque [Opens in a new window]
Abbas Askar
Affiliation:
Lund Observatory, Department of Astronomy, and Theoretical Physics, Lund University, Box 43, SE-221 00 Lund, Sweden email: askar@astro.lu.se
Mirek Giersz
Affiliation:
Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, ul. Bartycka 18, 00-716 Warsaw, Poland emails: mig@camk.edu.pl, agostino@camk.edu.pl
Manuel Arca Sedda
Affiliation:
Astronomisches Rechen-Institut, Zentrum für Astronomie, University of Heidelberg, Mönchhofstrasse 12-14, 69120, Heidelberg, Germany email: m.arcasedda@gmail.com
Ammar Askar
Affiliation:
School of Computer Science, College of Computing, Georgia Institute of Technology,801 Atlantic Dr, Atlanta, GA30332, USA email: aaskar3@gatech.edu
Mario Pasquato
Affiliation:
INAF, Osservatorio Astronomico di Padova, vicolo dell’Osservatorio 5, 35122 Padova, Italy email: mario.pasquato@inaf.it
Agostino Leveque
Affiliation:
Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, ul. Bartycka 18, 00-716 Warsaw, Poland emails: mig@camk.edu.pl, agostino@camk.edu.pl
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Abstract

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Sizeable number of stellar-mass black holes (BHs) in globular clusters (GCs) can strongly influence the dynamical evolution and observational properties of their host cluster. Using results from a large set of numerical simulations, we identify the key ingredients needed to sustain a sizeable population of BHs in GCs up to a Hubble time. We find that while BH natal kick prescriptions are essential in determining the initial retention fraction of BHs in GCs, the long-term survival of BHs is determined by the size, initial central density and half-mass relaxation time of the GC. Simulated GC models that contain many BHs are characterized by relatively low central surface brightness, large half-light and core radii values. We also discuss novel ways to compare simulated results with available observational data to identify GCs that are most likely to contain many BHs.

Keywords

stellar dynamicsglobular clusters: generalstars: black holes

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